Download Paush – Indication of Weather Here I would like to

Paush – Indication of Weather
Here I would like to quote an example of “Pausha” Paush month has been declared as
unauspicious for all religious functions because the hourly weather condition change in
Paush. If you keep a track of these weather conditions. We can understand the daily
weather of the complete year Paush to Margashirsha. It has got a significance to the
motion of Sun & Moon along with the rotation of earth. * This has base of
Astromathematies.
EXPLANATION :
The figure is drawn on the supposition that the earth (E) is in
the center, that the sun moves in the ecliptic, and the
precession of the equinoxes is caused by the motion of the
Ecliptic. With a given Nakshatra at the vernal equinox, we
can here at once find what Nakshatras would be at the other
cardinal points and hence also the month at the winter
(Fig.1)
solstice.
(Ref – Orayan by Lokmanya Tilak – Page 200)
Parameters of Observation :
For these we must have hourly observations of
1. Wind
-
its direction & speed.
2. Clouds
-
Their types, shapes & colours, and
direction in which the clouds are seen.
3. Lighting
-
Colour, shape & direction.
4. Thunder
-
Roaring sound or otherwise
5. Alpa Vrusti
-
Drizzling of rain, shower, or otherwise any.
Additional observations such as chanting of birds, change in natural behavior of
animals, etc.
*
30 days of Pousha
x
24 hrs. =
720 hours
Sun rotates through 12 Rashies where in he takes for 360 days
720
÷
360
=
2 hours represent a day
Accordingly starting from Poush every month is represented by two & half days (Tithi)
these simple calculation give us the exact day & time of rainfall.
The Earth’s Orbit
The earth is a planet revolving around the sun
in an elliptical path or orbit, the sun being situated at
a focus S of the ellipse (Fig.-2) This is a Kepler’s
first law of planetary motion. The time required for
the earth to make a complete revolution of its orbit is
a year. As the earth progresses in its orbit, the
direction of the earth, as viewed from the sun, is continually altering; the angular velocity
is, however, not uniform. Since our observations are made from the earth, then relative
to the earth the sun appears to describe an elliptical orbit around the earth.
In (fig. 3) C is the centre of the earth and the
ellipse represents the apparent to describe an elliptical
orbit of the sun relative to the earth. The sequence of
positions of the sun, namely a, e, f, b, g in this orbit,
corresponds to the sequence of positions A, E, F, B, G
of the earth in its orbit round the sun (Fig. 2). In the
course of the year, the sun thus appears to make a complete circuit of the heavens against
the background of the stars. The plane of the orbit is called the plane of the ecliptic, and
the great circle in which this plane intersects the celestial sphere, whose centre is earth’s
centre C, is called the ecliptic.
In fig. 4, Let C be the centre of the celestial sphere on which the celestial equator
TϒR and the north pole P are drawn. We may imagine
that the stars can be viewed from the centre of the earth
that is, from C and accordingly they will occupy
definite positions on the celestial sphere in fig. 4. With reference to the stars, the plane of
the ecliptic will have a definite position and, consequently, the ecliptic will be a particular
great circle, which is found from observations to be inclined at an angle of about 23 ½o to
the celestial equator. In Fig. 4, YϒMU represents the ecliptic and its inclination to the
celestial equator is MϒR, which is known as the obliquity of the ecliptic.
Relative to the earth, the sun appears to move on the celestial sphere along the ecliptic –
in the direction YϒM – and twice yearly, at ϒ and M and between M and U the sun is on
the north pole side of the equator; its declination is then north. Similarly between U and
Y and between Y and ϒ its declination is south. The position ϒ, at which the sun’s
declination changes from south to north, is the vernal equinox. It is in this way that the
reference point ϒ, from which are measured the right ascensions of the stars, is obtained.
Thus if X is a star, its right ascension is ϒD or a measured along the equator from ϒ
eastwards, and its declination δ is DX. From the diagram it is seen that the right
ascension and declination of the sun are both changing continually. When the sun is at ϒ,
its right ascension and declination are both zero (this occurs about March 21 – the vernal
equinox); at M the right ascension is 6th and declination about 23 ½o N (this occurs about
June 21 – the summer solstice); at U the right ascension is 12th and declination 0o (this
occurs about September 21 – the autumnal equinox) and at Y the right ascension is 18th
and the declination about 23 ½o S(this occurs about December 21 – the winter solstice).
(Ref. Spherical Astronomy by W.M. SMART. Chapter II Art. 25 Page 38-39)
compilation by : Sudhakar Raghunath Joshi, Deolali Camp, Nashik 422 401.
Email : [email protected]